Hydrodynamical models and synthetic spectra of circumstellar dust shells around AGB stars. I. Stationary solutions. J/A+AS/126/39 J/A+AS/126/39 Models of circumstellar dust shells Hydrodynamical models and synthetic spectra of circumstellar dust shells around AGB stars. I. Stationary solutions. M Steffen R Szczerba A Men'shchikov D Schoenberner Astron. Astrophys. Suppl. Ser. 126 39 1997 1997A&AS..126...39S Models, evolutionary circumstellar matter dust, extinction hydrodynamics radiative transfer stars: AGB and post-AGB stars: mass-loss Main properties of the steady state hydrodynamical models of circumstellar gas/dust shells around late type giants, computed for different stellar parameters (mass, luminosity, effective temperature) and dust composition (astronomical silicates, graphite, or amorphous carbon, with properties given in Tab.1 and Fig.1). Each table lists the results as a function of the adopted mass loss rate for fixed stellar parameters and dust properties. Tables 2 - 11 are related to Figures 2 - 11: Each of the figures shows the velocity structure and the resulting spectral energy distribution for a subset of models listed in the respective table.
Models results (table2-11) Model Model name number=1 the models are: C1 to C6 models: M= 1, L=1E4, Teff=3000, Astr. silicates, u1=2 km/s (Table2) D1 to D5 models: M= 4, L=5E4, Teff=2500, Astr. silicates, u1=2 km/s (Table3) E1 to E5 models: M=10, L=4E5, Teff=2500, Astr. silicates, u1=4 km/s (Table4) F1 to F4 models: M=30, L=1E4, Teff=2500, Astr. silicates, u1=4 km/s (Table5) G1 to G6 models: M= 1, L=1E4, Teff=2000, Graphite, u1=2 km/s (Table6) H1 to H6 models: M= 3, L=5E4, Teff=2000, Graphite, u1=2 km/s (Table7) I1 to I5 models: M= 5, L=5E4, Teff=2000, Graphite, u1=2 km/s (Table8) J1 to J6 models: M= 1, L=1E4, Teff=2000, Amorphous carbon, u1=2 km/s(Table9) K1 to K6 models: M= 3, L=5E4, Teff=2000, Amorphous carbon, u1=2 km/s(Table10) L1 to L5 models: M= 5, L=5E4, Teff=2000, Amorphous carbon, u1=2 km/s(Table11) Where M is Mstar (M_{sun}_), L is Lstar (L_{sun}_) , and u1 is the initial velocity (gas and dust) at the inner boundary r1. --- n_Model Note on Model number=2 For each mass loss rate, the second row (n_Model = n) lists the corresponding results from a model calculation ignoring gas pressure. Missing data indicate that no steady state solution was found. --- MassLoss Mass loss rate solMass/yr r1 Dust condensation radius 10+14cm l_r1/r* Limit flag on r1/r* --- r1/r* r1 in stellar radii --- l_ue Limit flag on ue --- ue Terminal gas outflow velocity km/s ue/vesc(r1) ue in units of escape velocity at r1 --- (w-u)/ue Terminal drift velocity in units of ue --- l_tauV Limit flag on tauV --- tauV Total optical depth at lambda 0.55 mum --- tau10 Total optical depth at lambda 10 mum --- tauF Flux-averaged total optical depth (Eq.25) --- Beta MassLoss*ue*c/L number=3 Beta = Mdot*ue*c/L = Ratio of momentum flux in the outflow to stellar photon momentum flux --- tables.texLaTeX version of the tables Matthias Steffen Ast. Inst. Potsdam Patricia Bauer CDS 1997Feb26Matthias Steffen <supas048@astrophysik.uni-kiel.de> J_A+AS_126_39.xml